There is no agreement on the thermal structure of the solar chromosphere. While results of the CO observations and 3D MHD simulations suggest very cool structures in the upper atmosphere, SUMER observations of UV spectral lines is interpreted as signature of a full-time hot chromosphere. We tried to look for cool structures in the solar

We report a re-brightening of the millisecond X-ray pulsar IGR J00291+5934. In August the source performed an outburst which was detected in X-ray, UV and optical (ATel #1660, #1664, #1665, #1666, #1667, #1668). Since then we have continued to monitor this source with the Faulkes Telescope North in many optical filters as it appeared to be fading

We have observed the accreting millisecond X-ray pulsar SAX J1808.4-3658 in its current outburst (ATel #1728, #1732, #1733) in the radio band with the Australia Telecope Compact Array (ATCA) on 2008 September 26th for about 5h (03:39 - 08:35 UT). The radio-counterpart was not detected. The 3-sigma upper-limits are 0.45 mJy/beam at 4.8 GHz and 0.72

Context: Hydrodynamical cosmological simulations predict flows of the intergalactic medium along the radial vector of the voids, approximately in the direction of the infall of matter at the early stages of the galaxy formation. Aims: These flows might be detected by analysing the dependence of the warp amplitude on the inclination of the galaxies

Photometric and spectroscopic data of the southern contact binary GSC04778-00152 are presented. Six new times of minimum are listed. For modelling purposes, we provide UBVRI phase diagrams of the contact binary with the contribution of the nearby companion removed.

The chromospheric temperature rise to values above the photospheric temperature cannot be due to radiative energy transport alone. We will outline different possibilities for the additional energy transport in the solar atmosphere by processes that require (or exclude) the presence of magnetic fields. We will discuss which of them could be